Astronomy:HD 192310

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Short description: Star in the constellation Capricornus
HD 192310
Location of HD 192310 (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Capricornus[1]
Right ascension  20h 15m 17.39138s[2]
Declination −27° 01′ 58.7116″[2]
Apparent magnitude (V) 5.73[3]
Characteristics
Evolutionary stage main sequence[4]
Spectral type K2+ V[5]
U−B color index 0.64[3]
B−V color index 0.88[3]
Variable type Suspected[6]
Astrometry
Radial velocity (Rv)−54.41±0.13[2] km/s
Proper motion (μ) RA: +1242.763[2] mas/yr
Dec.: −181.175[2] mas/yr
Parallax (π)113.4872 ± 0.0516[2] mas
Distance28.74 ± 0.01 ly
(8.812 ± 0.004 pc)
Absolute magnitude (MV)6.0[7]
Details
Mass0.83+0.07
−0.01[8] M☉
Radius0.83±0.02[8] R☉
Luminosity0.42+0.03
−0.02[8] L☉
Surface gravity (log g)4.38±0.19[9] cgs
Temperature5108+61
−60[8] K
Metallicity [Fe/H]−0.01±0.05[9] dex
Rotation47.7±4.9[10] days
Rotational velocity (v sin i)<3[10] km/s
Age7.5–8.9[7] Gyr
Other designations
5 G. Capricorni, CD−27°14659, GCTP 4804.00, Gl 785, HD 192310, HIP 99825, HR 7722, LHS 488, LTT 8009, NSV 12933, SAO 189065
Database references
SIMBADdata
Exoplanet Archivedata
ARICNSdata

HD 192310 (also known as 5 G. Capricorni or Gliese 785) is a star in the southern constellation of Capricornus. It is located in the solar neighborhood at a distance of 28.7 light-years (8.8 parsecs), and is within the range of luminosity needed to be viewed from the Earth with the unaided eye. (According to the Bortle scale, it can be viewed from dark suburban skies.) HD 192310 is suspected of being a variable star, but this is unconfirmed.

Description

This is a K-type main sequence star with a stellar classification of K2+ V.[5] HD 192310 has 83% of the mass and radius of the Sun. The effective temperature of the photosphere is 5108 K,[8] giving it the orange-hued glow of a K-type star.[11] It is older than the Sun, with age estimates in the range 7.5–8.9 billion years.[7] The proportion of elements other than hydrogen and helium, known as the metallicity, is similar to that of the Sun.[9] It is spinning slowly, completing a rotation roughly every 48 days.[10]

The space velocity components of this star are (U, V, W) = (–69, –13, –14) km/s. It is following an orbit through the Milky Way galaxy that has an orbital eccentricity of 0.18 at a mean galactocentric distance of 8.1 kpc.[12] The star will achieve perihelion in around 82,200 years when it comes within 20.18 ly (6.188 pc) of the Sun.[13]

Planetary system

The system has a Neptune-mass planet "b", discovered in 2010.[4] A second planet "c" was found in this system in 2011 by the HARPS GTO program, along with the now-doubtful HD 85512 b and the planets of 82 G. Eridani. The uncertainty in the mass of the second planet was much higher than for the first because of the lack of coverage around the full orbit. Both planets may be similar in composition to Neptune. They are orbiting along the inner and outer edges of the habitable zone for this star.[10][14]

A study in 2023 updated the parameters of these two planets, and identified a number of additional radial velocity signals. While most of these signals were attributed to stellar activity, one was considered a planet candidate. If real, this third planet would be a super-Earth orbiting closer to the star than the two known planets.[15]: 31  However, another 2023 study did not find this candidate signal and also attributed it to stellar activity.[16]: 10 

The HD 192310 planetary system[16]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥16.1±0.7 M⊕ 0.32±0.01 74.25±0.04 0.11±0.02 — —
c ≥15.9±0.9 M⊕ 1.21±0.02 534.9+5.9
−5.1 		0.06+0.05
−0.04 		— —

See also

References

  1. ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific 99 (617): 695. doi:10.1086/132034. Bibcode: 1987PASP...99..695R  Constellation record for this object at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 Johnson, H. L. et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory 4 (99): 99, Bibcode: 1966CoLPL...4...99J 
  4. ↑ 4.0 4.1 Howard, Andrew W. et al. (March 2011), "The NASA-UC Eta-Earth Program: III. A Super-Earth orbiting HD 97658 and a Neptune-mass planet orbiting Gl 785", The Astrophysical Journal 730 (1): 10, doi:10.1088/0004-637X/730/1/10, Bibcode: 2011ApJ...730...10H 
  5. ↑ 5.0 5.1 Gray, R. O. et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal 132 (1): 161–170, doi:10.1086/504637, Bibcode: 2006AJ....132..161G 
  6. ↑ Samus, N. N. et al. (2009), "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)", VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1: B/GCVS, Bibcode: 2009yCat....102025S 
  7. ↑ 7.0 7.1 7.2 Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal 687 (2): 1264–1293, doi:10.1086/591785, Bibcode: 2008ApJ...687.1264M 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 Harada, Caleb K. et al. (June 2024), "Setting the Stage for the Search for Life with the Habitable Worlds Observatory: Properties of 164 Promising Planet-survey Targets", The Astrophysical Journal Supplement Series 272 (2): id. 30, doi:10.3847/1538-4365/ad3e81, Bibcode: 2024ApJS..272...30H 
  9. ↑ 9.0 9.1 9.2 Ecuvillon, A. et al. (May 2004), "Nitrogen abundances in planet-harbouring stars", Astronomy and Astrophysics 418 (2): 703–715, doi:10.1051/0004-6361:20035717, Bibcode: 2004A&A...418..703E 
  10. ↑ 10.0 10.1 10.2 10.3 Pepe, F. et al. (2011), "The HARPS search for Earth-like planets in the habitable zone", VizieR On-line Data Catalog: J/A+A/534/A58 534: pp. A58, doi:10.1051/0004-6361/201117055, Bibcode: 2011yCat..35340058P 
  11. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html, retrieved 2012-01-16 
  12. ↑ Porto de Mello, Gustavo; del Peloso, Eduardo F. (April 2006), "Astrobiologically Interesting Stars Within 10 Parsecs of the Sun", Astrobiology 6 (2): 308–331, doi:10.1089/ast.2006.6.308, PMID 16689649, Bibcode: 2006AsBio...6..308P 
  13. ↑ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics 575: 13, doi:10.1051/0004-6361/201425221, A35, Bibcode: 2015A&A...575A..35B 
  14. ↑ Schneider, Jean, HD 192310 c, http://exoplanet.eu/planet.php?p1=HD+192310&p2=c, retrieved 2011-10-29 
  15. ↑ Laliotis, Katherine et al. (April 2023), "Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions", The Astronomical Journal 165 (4): 176, doi:10.3847/1538-3881/acc067, Bibcode: 2023AJ....165..176L 
  16. ↑ 16.0 16.1 Cretignier, M. et al. (August 2023), "YARARA V2: Reaching sub-m s−1 precision over a decade using PCA on line-by-line radial velocities", Astronomy & Astrophysics 678: A2, doi:10.1051/0004-6361/202347232, Bibcode: 2023A&A...678A...2C 



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